Calendar time - Rekihyoji

Japanese: 暦表時 - れきひょうじ
Calendar time - Rekihyoji

A time system measured based on the revolution of the Earth. It is called orbital time, as opposed to rotation time, which is based on the rotation of the Earth. At the 8th General Assembly of the International Astronomical Union in 1952, calendar time was defined as the sidereal year, which is the revolution period of the Earth, but in 1955 the same assembly decided to adopt the solar year, which has a more fundamental meaning than the sidereal year, and the 10th General Assembly of the International Committee for Weights and Measures in 1956 adopted the calendar second as the unit of time. Calendar time is a time system in which celestial mechanics based on the law of gravitation holds true, and if calendar time is used, the positions of the Sun, Moon, planets, and other celestial bodies should be observed at the positions indicated in the celestial ephemeris table, but in reality, they are observed according to universal time, which is the time of rotation, so the positions of celestial bodies differ by the difference between universal time and calendar time. It is difficult to obtain the correction value for the difference between calendar time and universal time by observing the movement of the Sun, and it can be obtained by observing the movement of the Moon, but this method takes time and is not useful for modern purposes. Therefore, the natural frequency of the cesium atomic standard is defined as the value for one second of ephemeris time, and the atomic time displayed by an atomic clock can be used as a proxy for ephemeris time.

[Toshio Watanabe]

[Reference item] | Atomic time | Hour | Second | Solar year

Source: Shogakukan Encyclopedia Nipponica About Encyclopedia Nipponica Information | Legend

Japanese:

地球の公転に基づいて測られる時系。地球の自転に基づく自転時に対して公転時といわれる。1952年国際天文学連合第8回総会で、地球の公転周期の恒星年をもって暦表時を定義したが、1955年の同総会は恒星年よりさらに基本的な意味をもつ太陽年を採用することにし、翌1956年の国際度量衡委員会第10回総会で暦表時の秒が時間の単位として採用された。暦表時は万有引力の法則に基づく天体力学が成り立つような時系であり、暦表時を使えば、太陽・月・惑星ほかの天体の位置は天体位置表の示す位置に観測されるはずであるが、実際には自転時である世界時によって観測するから、世界時と暦表時の差だけ天体の位置は違ってくる。暦表時と世界時のずれの修正値は、太陽の運行の観測から求めることは困難で、月の運行の観測から求められるが、この方法では時間がかかり、現在の用に役だたない。そのためセシウム原子標準の固有振動数が暦表時の1秒に対する値として定められており、原子時計が表示する原子時によって暦表時を代行させることができる。

[渡辺敏夫]

[参照項目] | 原子時 | | | 太陽年

出典 小学館 日本大百科全書(ニッポニカ)日本大百科全書(ニッポニカ)について 情報 | 凡例

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